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| 1 | 关键天体反应18Ne(α,p)21Na的实验研究显示文摘在X射线暴高温高密度的环境中,18Ne(α,p)21Na很可能是由热CNO循环突破到rp过程的一个重要反应。到目前为止,人们测得的反应率还存在很大的不确定性。实验中用CRIB(CNS Radioactive Ion Beam separator)提供的21Na放射性束轰击8.8 mg/cm2的聚乙烯厚靶,利用放置在θlab=-14°,0°,14°处的3套硅条探测器望远镜阵列对反冲轻粒子进行鉴别和测量,测得在一段能区(Ex=5.5~9.2MeV)内21Na(p,p)21Na的激发函数。通过对21Na(p,p)共振弹性散射截面进行R矩阵拟合,得到了22Mg共振能级的自旋宇称以及质子宽度等信息,从而为计算18Ne(α,p)21Na反应率提供了实验参数。 | 张立勇 许世伟 何建军 H.Yamaguchi S.Kubono Y.Wakabayashi: 陈思泽 胡钧 马朋 Y.Togano T.Hashimoto D.Kahl T.Teranishil 陈若富 王宏伟 田文栋 郭冰 S.Hayakawa N.Iwasa T.Yamada T.Komatsubara | 2013 | 原子核物理评论2013，30，4： | 1 |
| 2 | Measurement of 2H(12N, 13O)n Angular Distribution and Determination of Astrophysical 12N(p, γ)13O Reaction Rate显示文摘The evolution of massive stars with very low-metallicities depends critically on the amount of CNO nuclides which they produce. The 12N(p, γ)13O reaction is an important branching point in the rap processes, which are believed to be alternative paths to the slow αp process for producing CNO seed nuclei and thus could change the fate of massive stars. In the present work, the angular distribution of | GUO Bing SU Jun LI Zhi-hong WANG You-bao YAN Sheng-quan LI Yun-ju SHU Neng-chuan HAN Yin-lu BAI Xi-xiang CHEN Yong-shou LIU Wei-ping H.Yamaguchi D.N.Binh T.Hashimoto S.Hayakawa D.Kahl S.Kubono HE Jian-jun HU Jun XU Shi-wei N.Iwasa N.Kume LI Zhi-huan | 2012 | Annual Report of China Institute of Atomic Energy2012，，1： | 0 |
| 3 | Resonant Scattering of 22Na+p by Thick-Target Inverse Kinematic Method显示文摘22 Na is one of the most important yet debatable cosmic γ-ray emitters. The relative short half-life of 22 Na (T1/2=2.6 a) and the delayed 1.275 MeV γ-ray indicate that the 22Na may be a very sensitive probe to the nova outburst, especially for the nearby ONe novae from the Sun. | WANG You-bao JIN Sun-jun SU Jun YAN Sheng-quan LI Yun-ju GUO Bing LI Zhi-hong BAI Xi-xiang LIU Wei-ping H.Yamaguchi S.Kubono D.Kahl J.Hu H.S.Jung J.Y.Moon T.Teranishi H.W.Wang H.Ishiyama H.Iwasa H.Komatsubara | 2012 | Annual Report of China Institute of Atomic Energy2012，，1： | 0 |
| 4 | Neutron and Alpha Structure in Neutron Deficient Nuclei in Astrophysics显示文摘The paper includes discussions on the important role of neutron and alpha configurations in proton-rich nuclei in nuclear astrophysics in terms of nucleosynthesis under extremely high-temperature hydrogenburning conditions. The νp-process, which is supposed to take place at the very early epoch of type II supernovae, has considerable neutrons and alphas together with protons. The alpha-induced reactions on proton-rich unstable nuclei in the light mass regions is expected to play a crucial role, but very few of them were investigated well yet because of the experimental difficulties. Specifically, I report our recent experimental effort for the breakout process from the pp-chain region,~7Be(α, γ)^(11)C(α,p)^(14)N under the νp-process. The neutron-induced reactions on proton-rich nuclei, which is even more a challenging subject, were investigated previously for very few nuclei. One possible experimental method is the Trojan Horse Method(THM). We successfully have applied THM to the ^(18)F(n,α)^(14)N reaction study with an unstable beam of ^(18)F. | S.Kubono 何建军 H.Yamaguchi D.M.Kahl S.Hayakawa T.Teranishi S.Cheribini M.Gulino Y.K.Kwon T.Hashimoto Y.Wakabayashi N.Iwasa S.Kato T.Komatsubara D.N.Binh L.H.Khiem N.N.Duy T.Kawabata C.Spitaleri G.G.Rapisarda M.La Cognata L.Lamia R.G.Pizzone S.Romano A.Coc N.de Sereville F.Hammache G.Kiss S.Bishop | 2016 | 原子核物理评论2016，33，2： | 0 |
| 5 | Research Progress of Nuclear Astrophysics Physics:Progress of Jinping Underground Laboratory for Nuclear Astrophysics Experiment JUNA显示文摘1 Progress of this program This program is supported by the China Jinping Underground Laboratory(CJPL)and the direct measurement of stellar key reactions of(α,γ),(α,n),(p,γ)and(p,α)will be precisely carried out at the merit of current project by utilizing high stability and intensity accelerator,high efficiency detector and the shielding of extremely low background. | LIU Wei-ping LI Zhi-hong HE Jian-jun TANG Xiao-dong LIAN Gang GUO Bing AN Zhu CHEN Qing-hao CHEN Xiong-jun CHEN Yang-ping CHEN Zhi-jun CUI Bao-qun DU Xian-chao FU Chang-bo GAN Lin HAN Zhi-yu HE Guo-zhu A.Heger HOU Su-qing HUANG Han-xiong HUANG Ning JIA Bao-lu JIANG Li-yang S.Kubono LI Jian-min LI Kuo-ang LI Tao LI Xin-yue LI Yun-ju M.Lugaro LUO Xiao-bing MA Shao-bo MEI Dong-ming QIAN Yong-zhong QIN Jiu-chang REN Jie SU Jun SUN Liang-ting TAN Wan-peng I.Tanihata WANG Peng WANG You-bao WU Qi XU Shi-wei YAN Sheng-quan YANG Li-tao YU Xiang-qing YUE Qian ZENG Sheng ZHANG Huan-yu ZHANG Hui ZHANG Li-yong ZHANG Ning-tao ZHANG Qi-wei ZHANG Tao ZHANG Xiao-peng ZHANG Xue-zhen ZHANG Zi-min ZHAO Wei ZHAO Zhuo ZHOU Chao ZHOU Yong | 2015 | Annual Report of China Institute of Atomic Energy2015，，1： | 0 |
| 6 | 核天体物理研究进展——基于锦屏深地实验室的核天体物理关键科学问题研究显示文摘1项目总体进展本项目总体思路是依托锦屏山深地实验室,通过优化高稳定高流强加速装置、高性能探测器和极低本底屏蔽等关键技术,开展恒星中关键的(α,γ)、(α,n)、(p,γ)和(p,α)反应的直接精确测量。通过设置4个反应课题,在锦屏深地核天体物理实验室JUNA直接测量4个最重要的核天体物理反应。通过设置一个实验技术课题,为前4个课题提供实验基础条件和实验技术支撑。项目计划5年完成,2015年是项目执行的第一年。 | 柳卫平 李志宏 何建军 唐晓东 连钢 郭冰 安竹 陈庆豪 陈雄军 谌阳平 陈治均 崔保群 杜先超 符长波 甘林 韩治宇 贺国珠 A.Heger 侯素青 黄翰雄 黄宁 贾宝路 江历阳 S.Kubono 李荐民 李阔昂 李涛 李鑫悦 李云居 M.Lugaro 罗小兵 马少波 梅东明 钱永忠 秦久昌 任杰 苏俊 孙良亭 谭万鹏 I.Tanihata 王鹏 王友宝 武启 许世伟 颜胜权 杨丽桃 于祥庆 岳骞 曾晟 张环宇 张辉 张立勇 张宁涛 张奇玮 张涛 张笑鹏 张雪珍 张子民 赵伟 赵茁 周超 周勇 | 2015 | 中国原子能科学研究院年报2015，，1： | 0 |
| 7 | Measurement of^(25)Al+p Resonant Scattering显示文摘Type I X-ray bursts are the most frequently observed thermonuclear explosions in nature[1].They take place on the surface of accreting neutron star in low-mass X-ray binary systems. | Hu Jun H.Yamaguchi Xu Shiwei Zhang Ningtao Ma Shaobo Ru Longhui Liu Enqiang Liu Tong S.Hayakawa Yang Lei H.Shimizu D.Kahl C.B.Hamill A.Murphy Su Jun Fang Xiao K.Chae M.Kwag S.Cha N.N.Duy N.K.Uyen D.Kim R.G.Pizzone M.La Cognata S.Cherubini S.Romano A.Tumino J.Liang A.Psaltis M.Sferrazza D.Kim S.Kubono | 2019 | IMP & HIRFL Annual Report2019，，1： | 0 |
| 8 | Study of Proton Resonances in ^(22)Mg by Resonant Elastic Scattering of ^(21)Na+p and Its Astrophysical Implication in ^(18)Ne(α,p) ^(21)Na Reaction Rate显示文摘Proton resonant states in 22Mg have been investigated by the resonant elastic scattering of 21Na+p. The 21Na beam with a mean energy of 4.00 MeV/u was separated by the CNS radioactive ion beam separator(CRIB) and bombarded a thick(CH2)n target. The energy spectra of recoiled protons were measured at scattering angles of θcm ≈172° and 146°,respectively. A new state at 7.06 MeV has been observed clearly and another new one at 7.28 MeV is tentatively identified due to its low statistics. The proton resonant parameters were deduced from an R-matrix analysis of the differential cross section data. The astrophysical resonant reaction rate for the 18Ne(α,p)21Na reaction has been estimated,and it is about five times larger than that assumed before. | S.Kubono T.Teranishi M.Notani H.Baba S.Nishimura J.Y.Moon M.Nishimura S.Michimasa H.Iwasaki Y.Yanagisawa N.Hokoiwa M.Kibe J.H.Lee S.Kato Y.Gono C.S.Lee | 2009 | 原子核物理评论2009，26，S1： | 0 |
| 9 | ~1H(^(17)F,α)^(14)O反应截面测量显示文摘^(14)O(α, p)^(17)F是天体X射线暴中重要的突破反应。本工作通过厚靶方法测量其逆反应~1H(^(17)F,α)^(14)O的反应截面来研究这一关键反应。本实验工作是在日本东京大学原子核科学研究中心(CNS)的低能次级束流线(CRIB)上完成的,后续的扣除本底实验是在兰州放射性束流线(RIBLL1)上完成的。CRIB实验是通过~2H(^(16)O,n)^(17)F转移反应产生^(17)F次级束,经过CRIB分离提纯之后,利用该次级束轰击氢气靶。在氢气靶后布置了三套望远镜探测器系统,用以探测不同实验角度的反冲α粒子,在数据处理的过程中经过动力学重构后得到了~1H(^(17)F,α)^(14)O反应在质心系能区E_(c.m.)=2.7~3.4 MeV的反应截面。实验结果在3 MeV以上的高能区与前人的薄靶实验数据是一致的,在低能区本工作获得了新的实验数据,倾向于支持干涉相消的理论预言结果。 | 贾宝路 胡钧 何建军 许世伟 H.Yamaguchi D.Kahl 马朋 苏俊 王宏伟 T.Nakao Y.Wakabayashi T.Teranishi K.I.Hahn J.Y.Moon H.S.Jung T.Hashimoto A.A.Chen D.Irvine C.S.Lee S.Kubono | 2019 | 原子核物理评论2019，36，1： | 0 |
| 10 | 2H(12N,13O)n角分布的测量以及12N(p,γ)13O反应率的确定显示文摘正大质量贫金属恒星的演化与其产生的CNO核数目紧密相关,快速αp俘获过程是产生CNO种子核的重要过程之一,它可改变大质量恒星的命运。12N(p,γ)13O反应是快速αp过程中的一个重要分支点。本工作首次测量了Ec.m.=8.4MeV的2H(12N,13O)n质子转移反应角分布。 | 郭冰 苏俊 李志宏 王友宝 颜胜权 李云居 舒能川 韩银录 白希祥 陈永寿 柳卫平 H.Yamaguchi D.N.Binh T.Hashimoto S.Hayakwa D.Kahl S.Kubono 何建军 胡钧 许世伟 N.Iwasa N.Kume 李智焕 | 2012 | 中国原子能科学研究院年报2012，，1： | 0 |
| 11 | 用逆运动学厚靶方法研究22Na+p共振散射显示文摘正22Na是最重要但又有争议的宇宙γ射线发射体之一,其相对较短的衰变寿命(T1/2=2.6a)及其缓发的1.275MeVγ射线,使其有可能成为太阳系附近ONe新星爆发的灵敏探针。在新星形成过程中随温度提高有两种模式,即20Ne(p,γ)21Na(β+)21Ne(p,γ)2Na或20Ne(p,γ)21Na(p,γ)22Mg(β+)22Na可生成22Na, | 王友宝 金孙均 苏俊 颜胜权 李云居 郭冰 李志宏 白希祥 柳卫平 H.Yamaguchi S.Kubono D.Kahl J.Hu H.S.Jung J.Y.Moon T.Teranishi H.W.Wang H.Ishiyama N.Iwasa H.Komatsubara | 2012 | 中国原子能科学研究院年报2012，，1： | 0 |
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